Ultraluminous X-ray pulsar: accreting magnetar? H. Tong ( 仝号 ) 2015.5 Xinjiang Astronomical Observatory, Chinese Academy of Sciences Homepage: www.escience.cn/people/tonghao Bachetti et al. 2014 In one ultraluminous X-ray source 10^40 erg s^-1 Pulsation (1.37 s) modulated By the orbital motion (2.5 day) Content 1. Introduction 2. Isolated magnetars 3. Accreting magnetars? History of pulsars 1967: discovery of pulsars (Hewish, Bell et al.) ~1970: X-ray pulsars (accreting neutron stars in binary systems, Giacconi et al.) 1982: millisecond pulsars (Backer et al. ) Recycled neutron stars via low mass X-ray binaries 1990s: magnetar (Thompson/Duncan, Kouveliotou et al.) Where are accreting magnetars? X-ray pulsars 1.Rotation-powered X-ray pulsars (Crab, Vela) 2.Accretion-powered X-ray pulsars (accreting NSs in XRBs) 3.Magnetars (AXPs/SGRs, neutron stars powered by their magnetic energy) 4.Thermal-powered X-ray pulsars (XDINSs, CCOs etc) Observational appearances of accreting magnetars? Magnetars my favorite! Tong & Wang 2014 Traditional magnetar model (Mereghetti 2008) Magnetar = 1. young NS (SNR & MSC) 13 2. Bdip> BQED=4.4×10 G (braking) 14 15 3. Bmul=10 -10 G (burst and super-Eddington luminosity and persistent emission) Giant flares of magnetars (Mereghetti 2008): 1. Spike+pulsating tail (hundreds of seconds) 2. 10^4 times super- Eddington during the tail (10^42 erg s^-1) Explanation: 10^15 G magnetic field as the energy power and cause of super- Eddington luminosity Restless magnetars: Woods+ 2007 bursts A period of enhanced spindown Restless magnetars PSR J1622-4950 (Levin+ 2012) Low magnetic field magnetar Bdip=7.5*10^12 G (Rea et al. 2010, 2012; Zhou et al. 2014) Timing and explanations: evolution? Tong & Xu 2012 ApJ Wind braking of magnetars: low-B for many magnetars Tong et al. 2013 ApJ Decreasing Pdot for the second low-B magnetar Tong & Xu 2013 RAA Scholz+ 2014 Spectra of magnetars (Abdo et al. 2010) Cutoff? 15 Cuttoff at ~130keV for 4U 0142+61 (Wang, Tong, Guo 2014 RAA; 9 years Integral data) Conclusion: ultra-relativistic models can be ruled out! The key difference between magnetars and rotation-powered pulsars: multipole magnetic field! Not their positions on the P-Pdot diagram (determined by the magnetospheric torque) Evidence for strong multipole field in accreting systems (Tong & Wang 2014): 1. magnetar burst 2. hard X-ray tail 3. ... Super slow X-ray pulsar may not be accreting magnetars (Tong & Wang 2014) Super slow X-ray pulsars in HMXBs Ultraluminous X-ray sources (Feng & Soria 2011) X-ray point sources offset from the nuclei of nearby galaxies Lx=10^39-10^41 erg s^-1 Intermediate mass black hole (100-10000 Msun) or super-Eddington accreting stellar mass black hole or ... Bachetti et al. 2014 Pulsation (1.37 s) modulated By the orbital motion (2.5 day) Bachetti et al. 2014 The neutron star is spinning up! Pdot=-2*10^-10 Typical accretion-power X-ray pulsars Problem & Difficulity: How to explain the super-Eddington luminosity (10^40 erg s^-1) and spin-up rate? Accreting magnetar Models: accreting magnetar Observation: Bachetti et al. (arXiv:1410.3590) 1. Eksi et al. (arXiv:1410.5205): accreting magnetar, smaller torque during accretion equilibrium 2. Lyutikov (1410.8745): accreting magnetar, smaller torque due to super-Eddington accretion 3. Tong (1411.3168): accreting low magnetic field magnetar 4. Christodoulou et al. (1411.5434): accreting normal neutron star 5. Dall'Osso et al. (1412.1834): accreting magnetar 6. Guo et al.: massive pulsars (GR responsible for the super Eddington luminosity) 7. Fragos et al. (1501.02679), Shao & Li (1502.03905): formation Accreting low magnetic field magnetar Aged magnetars are more like to be low magnetic field magnetars (10^6 yrs old; consistent with population synthesis) Super-Eddington luminosity due to the presence of strong multipole field (e.g.,10^14 G) Rotational behaviors due to the interaction of much lower dipole field (10^12 G) with the accretion flow Discussion • M82 X-2 may be the counterpart of this ultraluminous X-ray pulsar. 1. Wide luminosity range 10^37-10^40 erg s^-1 (Feng et al. 2007; Kong et al. 2007): due to switches between accretion phase and propeller phase 2. A disk component (at 4.1 sigma level, Feng et al. 201 0): – temperature (0.17+-0.03 keV) vs. 0.15 keV(theory), inner – disk radius (3.5+3.0-1.9)*10^9 cm vs. 7.5*10^7 cm (theory) – future more accurate observations may contrain current models Discussion 3. Theoretical period range: 0.1-10^3 seconds for accreting magnetars. In search of these periodic signals, the orbital effect must be taken into consideration. 4. Three observational signatures of accreting ma gnetars (effect of multipole field): (1) magnetar- like burst; (2) A hard X-ray tail (>100keV); (3) ultraluminous X-ray pulsar. Summary • Ultraluminous X-ray pulsar as accreting magnetars 1. Magnetar strength multipole field (10^14 G)--> super- Eddington luminosity 2. Lower large scale dipole field (10^12 G) determines th e interaction between accretion flow and central neutr on star--> timing behaviors 3. Possible transient counterpart: switches between accretion phase and propeller phase 4.Wide theoretical period range 5.Three observational signatures of accreting magnetars The hard X-ray modulation telescope (HXMT) may contribute on these aspects.